Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 447, Issue 1, Pages 178-201Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu2400
Keywords
methods: numerical; galaxies: evolution; galaxies: formation
Categories
Funding
- University-of-Trieste/CINECA
- ISCRA
- PRIN MIUR grant 'The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid'
- PRIN-MIUR grant 'Evolution of Cosmic Baryons'
- PRIN-INAF grant 'The Universe in a Box: Multi-scale Simulations of Cosmic Structures'
- INFN 'INDARK' grant
- European Commission's FP7 Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356]
- University of Trieste
- 'Consorzio per la Fisica' of Trieste
- DFG Cluster of Excellence 'Origin and structure of the Universe'
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We present results of cosmological simulations of disc galaxies carried out with the GADGET-3 TreePM+SPH code, where star formation and stellar feedback are described using our MUlti Phase Particle Integrator model. This description is based on a simple multiphase model of the interstellar medium at unresolved scales, where mass and energy flows among the components are explicitly followed by solving a system of ordinary differential equations. Thermal energy from supernovae is injected into the local hot phase, so as to avoid that it is promptly radiated away. Akinetic feedback prescription generates the massive outflows needed to avoid the overproduction of stars. We use two sets of zoomed-in initial conditions of isolated cosmological haloes with masses (2-3) x 10(12) M-circle dot, both available at several resolution levels. In all cases we obtain spiral galaxies with small bulge-over-total stellarmass ratios (B/T similar to 0.2), extended stellar and gas discs, flat rotation curves and realistic values of stellar masses. Gas profiles are relatively flat, molecular gas is found to dominate at the centre of galaxies, with star formation rates following the observed Schmidt-Kennicutt relation. Stars kinematically belonging to the bulge form early, while disc stars show a clear inside-out formation pattern and mostly form after redshift z = 2. However, the baryon conversion efficiencies in our simulations differ from the relation given by Moster et al. at a 3 sigma level, thus indicating that our stellar discs are still too massive for the dark matter halo in which they reside. Results are found to be remarkably stable against resolution. This further demonstrates the feasibility of carrying out simulations producing a realistic population of galaxies within representative cosmological volumes, at a relatively modest resolution.
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